| Home | Trees | Indices | Help |
|---|
Galaxy luminosity functions (Schechter functions).
The LFHistory class implements a luminosity function history, encapsulating the changes in the galaxy luminosity distribution parameters as a function of redshift.
{},
wavelength=1500.0){'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6], 'alpha': [-1...,
extrap_var='t',
maglim=-19.252574989159953,
z_max=20.0,
skipIon=True){'MStar': -20.98, 'alpha': -1.73, 'phiStar': 0.0013...{'MStar': -20.64, 'alpha': -1.66, 'phiStar': 0.001,...{'MStar': -20.24, 'alpha': -1.74, 'phiStar': 0.0014...{'MStar': -19.3, 'alpha': -1.74, 'phiStar': 0.0014,...{'MStar': -19.9, 'alpha': -1.77, 'phiStar': 0.0014,...{'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6], 'alp...{'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6]...array([ 3.8, 5. , 5.9, 7.3, 9. ])
{'MStar': array([-21.072, -20.64 , -20.316, ...{'MStar': [-20.9, -20.55, -20.0, -19.7, -19.55], '...'cosmolopy'Use Labbe et al. (2009) relation between stellar mass and SFR.
See arXiv:0911.1356v4
Use Labbe et al. (2009) relation between stellar mass and SFR.
See arXiv:0911.1356v4
Use Kennicutt (1998) conversion from UV luminosity to star formation rate.
The SFR in Msun/year.
Kennicutt (1998ARA&A..36..189K) says:
SFR/(MSun/year) = 1.4 * 10^-28 (L_nu/ergs s^-1 Hz^-1)
where L_nu is the UV luminosity anywhere between 1500-2800 Angstroms.
Use Kennicutt (1998) conversion from UV luminosity to star formation rate.
Kennicutt (1998ARA&A..36..189K) says:
SFR/(MSun/year) = 1.4 * 10^-28 (L_nu/ergs s^-1 Hz^-1)
where L_nu is the UV luminosity anywhere between 1500-2800 Angstroms.
Use Kennicutt (1998) conversion from UV luminosity to AB magnitude.
Convenience function: uses L_nu_from_sfr and magnitudes.magnitude_AB_from_L_nu.
Integrate luminosity in galaxies above luminosity=L.
Uses an analytical formula.
Integrate luminosity in galaxies brighter than magnitudeAB.
Uses an analytical formula.
Integrate total luminosity in galaxies.
Uses an analytical formula.
Integrate total luminosity in galaxies.
Uses an analytical formula.
{},
wavelength=1500.0)
Ionizing photon rate density from a luminosity function.
in units of photons s^-1.
Given schecterParams, the parameters of a Schechter luminosity function (in terms of AB Magnitudes), sedParams, the parameters of the galactic Spectral Energy Distribution, and the wavelength of the AB Magnitudes, calculate the emission rate density of ionizing photons.
BrokenPowerlawSED
schechterTotLM
{'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6], 'alpha': [-1...,
extrap_var='t',
maglim=-19.252574989159953,
z_max=20.0,
skipIon=True)
Plot evolution of luminosity function params and total luminsity.
Schechter function at each redshift is integrated up to maglim to find total luminsity.
{'MStar':-20.98,'alpha':-1.73,'phiStar':0.0013,'z':3.8}
{'MStar':-20.64,'alpha':-1.66,'phiStar':0.001,'z':5.0}
{'MStar':-20.24,'alpha':-1.74,'phiStar':0.0014,'z':5.9}
{'MStar':-19.3,'alpha':-1.74,'phiStar':0.0014,'z':7.4}
{'MStar':-19.9,'alpha':-1.77,'phiStar':0.0014,'z':6.8}
{'MStar':[-20.98,-20.64,-20.24,-19.8,-19.6],'alpha':[-1.73,-1.66,-1.74,-1.74,-1.74],'phiStar':[0.0013,0.001,0.0014,0.0011,0.0011],'z':[3.8,5.0,5.9,7.3,9.0]}
{'MStar':[-20.98,-20.64,-20.24,-19.8,-19.6],'alpha':[-1.74,-1.74,-1.74,-1.74,-1.74],'phiStar':[0.0011,0.0011,0.0011,0.0011,0.0011],'z':[3.8,5.0,5.9,7.3,9.0]}
{'MStar':array([-21.072, -20.64 , -20.316, -19.812, -19.2 ]),'alpha':[-1.74,-1.74,-1.74,-1.74,-1.74],'phiStar':[0.0011,0.0011,0.0011,0.0011,0.0011],'z':array([ 3.8, 5. , 5.9, 7.3, 9. ])}
{'MStar':[-20.9,-20.55,-20.0,-19.7,-19.55],'alpha':[-1.57,-1.63,-1.84,-1.9,-1.999],'phiStar':[0.0013,0.0015,0.001,0.0006,0.00022],'z':[4.0,5.0,7.0,8.0,9.0]}
| Home | Trees | Indices | Help |
|---|